The He$\rm_{II}$ Fowler lines and the O$\rm_{III}$ and
N$\rm_{III}$ Bowen fluorescence lines in the symbiotic nova RR Telescopii

Selvelli, P. L.; Danziger, John; Bonifacio, P.

doi:10.1051/0004-6361:20066175

Cited by 26 publications

(39 citation statements)

References 63 publications

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“…The continuum in the region around λ 1640 Å is stronger by a large factor than around λ 4686 Å, resulting in a reduction of the contrast between the line and the continuum that may mask the λ 1640 Å emission. Selvelli et al 2007). Instead, the level 3 of He ii, which is the lower level of the 4686 line, is not affected by overpopulation and reabsorption.…”

Section: The Uv Emission Linesmentioning

confidence: 90%

“…Neither this method nor the method of continuum fitting with stellar atmosphere models can be applied to old novae to determine extinction because of the lack of any reference standard, and because models are still quite rudimentary. Another method employs ratios of recombination lines or of emission lines arising from a common upper level (see for example Selvelli et al 2007), but this is not applicable in our spectra on account of the lack of suitable emission lines. However, the UV range is the one most sensitive to the effects of the presence of reddening, since it is characterized by the presence of a broad interstellar (IS) absorption bump in the SED curve, centered near λ 2175 Å.…”

Section: The Reddening Correctionmentioning

confidence: 99%

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An archive study of 18 old novae

Selvelli

Gilmozzi

2013

A&A

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Aims. We present an overview of the UV spectral properties of old novae as a class. The data and results of this paper, together with data from the outburst phases, will be utilized in a follow-up study to determine statistical properties and to investigate correlations among the physical parameters of the quiescent and eruptive phases. Methods. All the available IUE, HST, and FUSE archive data for 18 old novae were used to derive accurate and homogeneous estimates of the reddening from the 2175 Å extinction bump and to determine the intrinsic spectral energy distribution corresponding to the utilization of both existing extinction curves. We also measured all the emission and absorption lines. Results. We have found good agreement between spectra taken at different epochs and by different instruments, a clear indication of the near constancy of the SED on timescales of several years. With the possible exception of GK Per, the dereddened UV continua are represented well by a single-curve power-law distribution F λ ∝ λ −α , with α in the range 0.32-2.55 for one curve and 0.35-2.88 for the other one. The extrapolation of the various UV power laws to the optical range yields values that are in good agreement with the V magnitudes. We interpret this result as evidence that the SED is dominated by the accretion disk in the UV and optical spectral regions. A detailed study of the emission spectrum has led to measuring and identifying more than one hundred features and to detecting several lines that are rather uncommon in other CVs and whose identification is uncertain.

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Section: The Uv Emission Linesmentioning

confidence: 90%

Section: The Reddening Correctionmentioning

confidence: 99%

An archive study of 18 old novae

Selvelli

Gilmozzi

2013

A&A

Self Cite

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“…This is in conflict with our identification of N iii λ4510. Additionally, O iii λ3133 should be roughly 3 times stronger than O iii λ3444 (McClintock et al 1975;Netzer et al 1985;Liu et al 1993;Kastner & Bhatia 1996;Selvelli et al 2007). This is not the case in our spectra, though the exact strengths are difficult to estimate because these are broad features and could be blended with other lines, such as [Ne v] λ3426.…”

Section: He and Metal Linesmentioning

confidence: 99%

To TDE or not to TDE: the luminous transient ASASSN-18jd with TDE-like and AGN-like qualities

Neustadt

Holoien

Kochanek

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present the discovery of ASASSN-18jd (AT 2018bcb), a luminous optical/UV/Xray transient located in the nucleus of the galaxy 2MASX J22434289-1659083 at z = 0.1192. Swift UVOT photometry shows the UV SED of the transient to be well modeled by a slowly shrinking blackbody with temperature T ∼ 2.5 × 10 4 K, a maximum observed luminosity of L max = 4.5 +0.6 −0.3 ×10 44 erg s −1 , and a total radiated energy of E = 9.6 +1.1 −0.6 × 10 51 erg. X-ray data from Swift XRT and XMM-Newton show a transient, variable X-ray flux with blackbody and power-law components. Optical spectra show strong, roughly constant broad Balmer emission as well as transient features attributable to He ii, N iii-v, O iii, and coronal Fe. While ASASSN-18jd shares similarities with Tidal Disruption Events (TDEs), it is also similar to the "rapid turn-on" events seen in quiescent galaxies and in faint Active Galactic Nuclei (AGNs).

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“…They are often interpreted in terms of the Bowen mechanism (see e.g., Selvelli et al 2007), where He ii Lyα overlaps with an O iii line and the resulting O iii cascade itself has a frequency that coincides with an N iii resonance line. The O iii Bowen lines below 4000 Å fall within a very noisy area of our VLT spectrum and cannot be identified.…”

Section: The Permitted Emission Linesmentioning

confidence: 99%

Disk evaporation in a planetary nebula

Gęsicki

Zijlstra

Szyszka

et al. 2010

A&A

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Aims. Binary interactions are believed to be important contributors to the structures seen in planetary nebulae (PN), and the sole cause of the newly discovered compact dust disks. The evolution of these disks is not clear, nor are the binary parameters required for their creation. Methods. Using HST imaging and VLT spectroscopy, both long-slit and integral field, we study the Galactic bulge planetary nebula M 2-29 for which a 3-year eclipse event of the central star has been attributed to a dust disk. Results. The central PN cavity of M 2-29 is being filled with a decreasingly, slow wind. An inner high density core is detected, of radius smaller than 250 AU, interpreted as a rotating gas/dust disk with a bipolar disk wind. The evaporating disk is argued to be the source of the slow wind. The central star is the source of a very fast wind (∼10 3 km s −1 ). An outer, partial ring is seen in the equatorial plane, expanding at 12 km s −1 . The azimuthal asymmetry is attributed to mass-loss modulation by an eccentric binary. A crucial point in disk evolution is represented by M 2-29 where ionization causes the gas to be lost, leaving a low-mass dust disk behind.

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The He$\rm_{II}$ Fowler lines and the O$\rm_{III}$ and N$\rm_{III}$ Bowen fluorescence lines in the symbiotic nova RR Telescopii

Cited by 26 publications

References 63 publications

An archive study of 18 old novae

An archive study of 18 old novae

To TDE or not to TDE: the luminous transient ASASSN-18jd with TDE-like and AGN-like qualities

Disk evaporation in a planetary nebula

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